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SAG 3: Planetary System Architecture and Dynamical Stability Rory Barnes (University of Washington) SAG chair: Brad Hansen Ravi Kopparapu Dave Bennet

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Page 1: SAG$3:$ Planetary$System$Architecture$ and$ Dynamical ... · SAG$3:$ Planetary$System$Architecture$ and$ Dynamical$Stability$ Rory$Barnes$ (University$of$Washington)$ SAG$chair:$Brad$Hansen$

SAG  3:  Planetary  System  Architecture  

and  Dynamical  Stability  

Rory  Barnes  (University  of  Washington)  

SAG  chair:  Brad  Hansen  Ravi  Kopparapu  Dave  Bennet  

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From  the  DC  meeGng  

How  well  does  one  need  to  characterize  planetary  architecture  to  properly  understand    exoplanet  habitability?  

Can  we  use  the  staGsGcal  properGes  of  planetary    systems  gleaned  from  a  GalacGc  census  to  inform    the  study  of  nearby  planetary  systems?    

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From  the  DC  meeGng  

Would  it  be  possible  or  prudent  to  exclude  some    nearby  systems  from  a  direct  imaging  target  list    based  on  prior  dynamical  informaGon  that  their    habitable  zones  are  unstable?  AlternaGvely,  is  it    advisable  to  prioriGze  a  target  list  based  on  such  dynamical  consideraGons?  

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What  is  “architecture”?  

Stellar  and  planetary  masses  Orbital  elements  “Minor  exoplanets”  Exo-­‐moons  Planet-­‐planet  interacGons    e.g.  mean  moGon  resonances  

ObliquiGes  

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Architecture  helps…  

Assess  planetary  habitability    -­‐  How  do  orbits  change  with  Gme?  

Determine  stability    -­‐  Where  should  we  NOT  look?  

Constrain  origins  scenarios    -­‐  Does  that  super-­‐Earth  have  water?  

Search  for  planets    -­‐  Fomalhaut  b    -­‐  T*V  

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Planetary    Habitability  

PerturbaGons  from  other  planets  change      orbits  with  Gme    obliquiGes  with  Gme  

   insolaGon  with  Gme    Gdal  effects  (mainly  for  M  stars)  

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HD  82943  

Barnes  &  Greenberg  2006  

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Planetary    Habitability  

Gl  581  w/extra  1  MJ    planet  at  0.75  AU  with  e  =  0.3  

red  is  planet  c  blue  is  planet  d  

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Planetary    Habitability  

Mutual  inclinaGons  -­‐>  fast,  large  obliquity        variaGons  on  terrestrial  planets  υ  And  c  and  d  have  relaGve  inclinaGon  of  30o    (McArthur  et  al.  2010)  

Moons  can  stabilize  obliquiGes,  but  are  they    detectable?  

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An  Earth    sandwiched  between  two    super-­‐Earths  with  mutual    inclinaGon  30o  

Figure  courtesy  John  Armstrong  

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Dynamical  Stability  

DetecGng  terrestrial  planets  is  hard  Can  we  narrow  our  search  by  excluding  some    habitable  zone  as  unstable?  

Several  studies:  Jones  et  al.  (2001);  Menou  &    Tabachnik  (2003);  Sandor  et  al.    (2005);  Kopparapu  &  Barnes  (2010)  

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Dynamical  Stability  

Kopparapu  &  Barnes    2010  

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Dynamical  Stability  

Kopparapu  &  Barnes    2010  

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Dynamical  Stability  

Kopparapu  &  Barnes    2010  

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Dynamical  Stability  

Kopparapu  &  Barnes    2010  

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Dynamical  Stability  

But…  Mean  moGon  resonances  can  stabilize  Earth-­‐mass  planets  can  masquerade  as      eccentricity  (Anglada-­‐Escude  et  al.  2010)  

Stability  analyses  should  be  used  cauGously  

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Planet  FormaGon  

Can  the  layout  of  a  planetary  system  reveal  its    history?  

Large  eccentriciGes  =>  planet-­‐planet  scamering  Mean  moGon  resonances  =>  migraGon  

Can  we  constrain  composiGon?  

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Planet  FormaGon  

Raymond,  Mandell  &  Sigurdsson    (2006)  

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DetecGon  

Kalas  et  al.  (2008)  

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DetecGon  

Barnes  et  al.  (2008)  

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DetecGon  

Transit  Timing  VariaGons  

Table  courtesy  Praveen  Kundurthy  

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Discussion